In the literature one does not find veiling determinations in the J band
for T Tauri
stars. Greene & Meyer (1995) and Casali & Eiroa (1996),
observed excess K emission in Young Stellar
Objects from near infrared intermediate spectral resolution
spectroscopy. They find that the observed sources are affected by
veiling emission from hot dust. Greene & Lada (1996) discuss
these results and find that rK
depends on the SED Class; Class III
sources have 
, Class II have
and
flat-spectrum sources have 
. These results were
obtained by combining spectroscopic and photometric data, with the
assumption that 
. The results
from the
observations presented here imply 
, which is high
compared to the value estimated (for Class II) by Greene & Lada
(1996). The assumption that 
is crucial for the
determination of rK by those
authors. If rJ has a mean
value near 0.56, as we observe, then using equations 5 and 6 in Greene
& Meyer (1995) one concludes that the mean rK is about 1.5,
which is in tune with the measurements presented here, that give a mean
rK of 1.3 with dispersion 0.9.